Quasinormal modes and shadow of noncommutative black hole

In this paper we investigate quasinormal modes (QNM) for a scalar field around a noncommutative Schwarzschild black hole. We verify the effect of noncommutativity on quasinormal frequencies by applying two procedures widely used in the literature. The first is the Wentzel–Kramers–Brillouin (WKB) approximation up to sixth order. In the second case we use the continuous fraction method developed by Leaver. Besides, we also show that due to noncommutativity, the shadow radius is reduced when we increase the noncommutative parameter. In addition, we find that the shadow radius is nonzero even at the zero mass limit for finite noncommutative parameter.

Initial studies for black hole perturbations were done by Regge and Wheeler 1 and Zerilli 2 for Schwarzschild geometry, as well as for the Kerr black hole 3 . In 1970 Vishveshwara 4 identified a type of disturbance subject to special conditions such as outgoing waves in the spatial infinity and ingoing waves in the vicinity of the event horizon. These disturbances were called quasinormal modes valid only for a group of complex frequencies 5 . These quasinormal frequencies present a real part that provides the oscillation frequency while the imaginary part determines the damping rate of the modes. The dominant quasinormal modes can be seen in gravitational wave signals and in this case, the emitted waves are related to many physical processes such as astrophysical phenomena involving the evolution of binary systems and stellar oscillations or other highly dense objects in the early universe. In this way these quasinormal modes have been observed experimentally by LIGO/VIRGO 6,7 .
The analysis of quasinormal modes has been widely explored in the literature [8][9][10][11][12][13][14][15][16][17][18] by using different mechanisms, such as the WKB approximation and numerical methods. The first works using the WKB approximation to find quasinormal modes were done by Schutz and Will 19 . Improvements in the method were made by Iyer and Will by adding corrections up to third order 20 , and so the results for Schwarzschild black hole are very close to those obtained by the numerical method of Leaver 21 in l ≥ 4 regime. Aiming at a new improvement in the WKB approach, studies made by Konoplya 22 extended the method up to sixth order leading to more accurate results. Currently, we can find extensions of the WKB approximation up to thirteenth order 23 . As aforementioned, the numerical method is another way to obtain quasinormal frequency modes. Therefore, the first numerical approach to calculate quasinormal frequencies was described by Leaver, and the applied mathematical procedure is called a continuous fraction 24 . In 21 , Leaver has obtained quasinormal modes for Schwarzschild and Kerr black holes and also for Reissner-Nordström black hole in 25 . Several works [26][27][28][29] have applied this numerical method that has presented a good precision.
In addition to quasinormal modes, in recent years several authors have devoted themselves to study the shadow of the black hole [30][31][32][33][34] . This shadow requires information about the geometry around the black hole, which makes its study a very important way to understand the properties near the event horizon. Moreover with the advancement and improvements of the experimental techniques allowed us the first image of a supermassive black hole in the center of the M87 galaxy by the Event Horizon Telescope 35,36 by using the properties of the shadow. These experimental results have been studied by several authors 37-39 stimulated by the possibility of understanding phenomena in the regime close to the event horizon.
In this work we will use the shadow ray to better understand the proximity of the noncommutative Schwarzschild black hole horizon. The noncommutative gravity has been extensively investigated, particularly in black hole physics, mainly due to the possibility of better understanding the final stage of the black hole-see [40][41][42][43] for further details. We know that there is a relationship between quasinormal modes and of the black hole shadow and that several investigations contributed to this understanding. One of the first studies that certainly served as a basis for structuring this relationship was made by Mashhoon 44 , which describes an alternative method to calculate quasinormal modes at the eikonal limit. The most detailed geodesics study is shown in Cardoso et al. 45 , which shows that the real part of the quasinormal modes is related to the angular velocity of the null circular orbit and the imaginary part is associated with the Lyapunov exponent. Stefanov et al. 46 in the eikonal regime established a connection between black hole quasinormal modes and lensing in the strong deflection limit.

Noncommutative black hole with Lorentzian smeared mass distribution
On this section we begin by considering a Lorentzian distribution 43,78 given by where θ is the noncommutative parameter of dimension length 2 and M is the total mass diffused throughout the region of linear size √ θ . Thus, the smeared mass distribution function becomes 58 Hence, the line element of the Schwarzschild black hole in the noncommutative background is now given by with where which represent the radius of the event horizon and the Cauchy horizon, respectively. The next step we consider the case of the massless scalar field described by the Klein-Gordon equation in the background (7) (1) where ω is the frequency and Y lm (ϑ, φ) are the spherical harmonics. Now, we can obtain a radial equation for R ωl (r): We can reduce the radial equation (12) into a Schrödinger like equation by introducing a new coordinate (called tortoise coordinate) given by dr * = f (r) −1 dr and so that the radial equation becomes where In the following sections, we will obtain the quasinormal frequencies by two methods that are widely used in the literature. The first uses a sixth order WKB approximation, and the second method introduced by Leaver and improved by Nollert 82 , consists of using the continuous fraction method to find numerically quasinormal modes. WKB approximation. Quasinormal modes correspond to solutions of the wave equation (14) that satisfy the conditions of the purely outgoing waves at infinity and purely incoming waves at the event horizon, i.e., In this section we will use the WKB approximation to find the quasinormal modes. The first works using the WKB approximation to evaluate the quasinormal modes were done by Schutz and Will 19 . Improvements in the method were made using corrections up to third order 20,79 and up to sixth order by Konoplya 22 . The quasinormal modes are obtained by using the sixth order corrections for the WKB approximation as follows where j are the correction terms of the model. We have that V eff is the maximum effective potential at point r * and ( ′′ ) refers to the second derivative with respect to the tortoise coordinate. We can obtain the values of r * by making V ′ eff = 0 . In Fig. 1 we show the curves of the effective potential for l = 1, 2 and = 0.0, 0.05, 0.10, 0.12 , i     Table 3. QN frequencies for l = 3.  Tables 1, 2 and 3 we present the tabulated quasinormal frequencies using sixth order WKB method.
Another possibility is to study scattering by using the WKB method done in 20 . In order to develop this investigation, we use the boundary conditions for Eq. (14) in the form: Notice that as we want to obtain the reflection and transmission coefficients, as done for tunneling in quantum mechanics, we need the condition A int = 0 . The quantity ω 2 − V eff in (14) is assumed to be purely real, and with these imposed conditions we can find where ω is purely real and � j (K) are coefficients that depend on the effective potential and K is a purely imaginary quantity. This way of studying scattering by using the WKB approximation can be also found in 23,80 . Thus, using the relationship between K and the reflection and transmission coefficients obtained in 20 we get the following: Now to find the coefficients, we just calculate the value K that can be obtained by solving the Eq. (19). This method has a good approximation for l > 0 as we can see in Fig. 2, where we have a comparison between the numerical results and the WKB approximation for the transmission coefficient for l = 1, 2, 3 and = 0.05, 0.12 . Notice that the curves obtained by the WKB approximation are very close to those obtained by the numerical method used in the paper 58 , showing that the method presents excellent results. The sixth-order WKB approximation does not show good results for l = 0 , improving only when we take large ω . This problem is also mentioned in 23 .
Leaver's continued fraction. The numerical method is another way to obtain the quasinormal frequency, and this procedure has been described by Leaver 21,25 , and which is also found in other works 26,27 showing that it is a method with good precision.
We start analyzing the radial equation (12) which is subject to boundary conditions at infinity r → ∞ and near the event horizon r → r + , such that one obtains the asymptotic solutions We can obtain a solution that has the desired behavior on the horizon ( r = r + ), and that can be written in the form By replacing the solution (23) in the Eq. (12), we obtain the recurrence relation and The recurrence relation coefficients α k , β k and γ k are simple functions of k and the parameters ω , l and the radius r − and r + : See that the solution (23) applied directly to the radial equation returns a three-term recurrence relation which makes it easier to use continued fractions. This is because our metric for a non-commutative black hole A int e −iωr * + A out e iωr * , r * → ∞, A tr e −iωr * , r * → −∞. www.nature.com/scientificreports/ results in a generalized spheroidal wave equation whose solutions are connected by three-term recurrence relations-see "Appendix" for further details. However, the Leaver's method is not necessarily limited to recurrence relations of this type as shown in 25 , where it was considered an equation that describes odd-parity perturbations of a charged black hole, which equation has series solutions whose coefficients are connected by four-term recurrence relations.
The boundary condition at infinity will be satisfied for quasinormal frequency values ω = ω n , so that the series in (23) is absolutely convergent. Hence, we have a recurrence relation with three terms to determine the coefficient a k , and we can write in terms of a continuous fraction 81 which can also be found as follows We can obtain the characteristic equation for quasinormal frequencies by assigning k = 0 in (30) and comparing with reason a 1 /a 0 = −β 0 /α 0 obtained from (24), With the equation above, we can obtain the quasinormal frequencies ω n , by just calculating its roots numerically. However, the Eq. (31) is more used to find the fundamental frequency in the case of the more stable root, and another way of finding the modes is to invert this equation to a large number of k as follows To complement the analysis, we will check the behavior for very large k, as done in 82 . Now, we have to reorganize the Eq. (25) dividing α , β and γ by a k to obtain We can see that, lim k→∞ (a k+1 /a k ) ≃ 1 , and we can get a more complete expression by expanding a k+1 /a k in power series in terms of √ k, By considering the series up to the third term and admitting C 0 = 1 we have Now, to obtain the values of C 1 and C 2 , we replace these two expressions above into Eq. (33) in the very large k regime by making the multiplications and restricting up to terms of the order k −3/2 to get such that we find the following: Now we have, Here, we see that at the limit r − → 0 and r + → 1 , we get the result for the Schwarzschild case initially found by Leaver.  Tables 1, 2 and 3, we present some results for the quasinormal modes computed using the sixth-order WKB approximation, and the Leaver's continues fraction method described in the previous section by admitting M = 1 for various values of � = √ θ/π , l and n. We see that the results between the methods approach when l > 1 , this is, due to the instability of the WKB method for small multipole numbers mainly close to zero this instability can also be seen in the graphs of Fig. 3. An important detail is in the sign of the imaginary part that is always negative when the frequency is associated with the scalar field. A justification for this is due to the exponential drop of the quasinormal modes over time by losing energy in the form of scalar waves.
We can see the influence in the quasinormal modes for the noncommutative case by admitting values for where = 0 returns to the Schwarzschild case. With the increase of the non-commutative parameter , we have an increase in the real part of the quasinormal frequency, while the imaginary part begins to grow and then decreases. Another way of visualizing the effects of the noncommutative parameter is through the graphs of Fig. 3, these plots were obtained using the WKB method. We have quasinormal modes where in the plot we depicted the real part (top) and the imaginary part (bottom). The modes are based on n for the following multipoles numbers l = 1, 2, 3 and 4, for which we see that the results become more linear with the results varying and l = 3 and 4. Thus, in Fig. 3 we observe that, by varying l and the parameter θ , the imaginary part of the frequency does not cross the horizontal axis or change sign, thus indicating that the black hole remains stable due to scalar perturbation. In addition, it is interesting to make a plot for the complex plane as in Fig. 4 where we consider three families of multipoles l = 1, 2, 3 and varying as follows 0 (black), 0.05 (red), 0.10 (blue), 0.12 (green). The left panel was obtained by the WKB approximation and the right panel by the continuous fraction method (numerical). We can see that the frequency curves incline more closely when we use the WKB approximation. We also see that for the extreme case = 0.12 the curve tilts more to the left in both methods.

Null geodesic and Shadow of a noncommutative black hole
We know that in the vicinity of a black hole all the photons are absorbed so that a distant observer looking at the black hole, in absence of any other source, will see a spot created by this absorption, and this spot is usually called the shadow of the black hole. These shadows have been studied long ago by Synge 83 and Luminet 84 who started studies for Schwarzschild black hole while Kerr black holes were studied by Bardeen 85 .
As these shadows correspond to the apparent shape of the photon capture orbits, the space-time metric itself is enough to determine them and thereby better understand the geometry of the near horizon. One method of Null geodesic. We can find the geodesics from Eq. (7) by taking a Lagrangian in the form Thus, we have where the " · " is the derivative with respect to an affine parameter. We are interested in the path of a ray of light in the described metric, which is spherically symmetrical, so if we analyze in a plane, any ray of light that begins with a certain angle ϑ must remain with the same angle. We will then consider an equatorial plane by setting the angle ϑ to π/2. Thus, two equations are enough to describe the movement of a beam of light. We can put together a system with these equations that give rise to two geodesic motion constants E and L, which correspond to energy and angular momentum respectively: Now, as our goal is to study the null geodesics we have to g µνẋ µẋν = 0 , and using the Eq. (43) we can write Introducing a new variable u = 1/r we can write the orbit equation as follows where b = L/E is the impact parameter defined as the perpendicular distance (measured at infinity) between the geodesic and a parallel line that passes through the origin. So differentiating (45) we have, By solving the Eqs. (45) and (46) numerically, we can obtain the behavior of the geodesic lines for different values of the impact parameter b. In the Fig. 5, we verify the change of the geodesic lines for different impact parameters b and also by varying the values of the noncommutative parameter. In the figures, we have a black disk that represents the limit of the event horizon, the internal dotted circle is the radius for the photon sphere (critical radius), and the external dashed circle is the critical impact parameter (shadow). Hence, we see that the noncommutative parameter decreases the effect of the black hole on the light beams. For a similar effect see also 93 . www.nature.com/scientificreports/ Critical orbit and shadows. It is known that the shadow of the black hole is directly related to the impact parameter for the photon orbit, as we will see below. So to determine the shadow limit, we will start by studying the effective potential that satisfies the equation of the null geodesic as follows where using (44), we have In this case, we can obtain a critical radius or critical circular orbit for a photon r c and critical impact parameter b c , by using the following conditions: V eff (r c ) = 0 and dV eff (r c ) dr = 0 . So we find Let us now compute the size of the black hole shadow that can be expressed via celestial coordinates as follows 85 where (r o , ϑ o ) is the observer position at infinity.
As our study is restricted to the equatorial plane, the radius that delimits the size of the shadow is equivalent to the critical impact parameter, and so we have where In a semiclassical description of the scattering 86 , the impact parameter is associated with each partial wave b = (l + 1/2)/ω in the large l regime. As shown in 45 , the real part of the quasinormal frequencies at the eikonal This suggests a relationship between quasinormal frequencies and shadow radius as done by Jusufi 47 at the eikonal limit, showing that the real part of quasinormal modes is inversely proportional to the radius R s as follows Note that this expression is valid only for large values of l in most of the cases although fails for Einstein-Lovelock theory as shown by Konoplya and Stuchlik 94 . We can see in Fig. 3 that the higher the value of l the smaller the contribution of n. Thus by using the results obtained by the WKB approximation we compare with the shadow radius R s .
In the Table 4 we see that by increasing the value of l, the results between the real part of the quasinormal frequencies and the black hole shadow radius approach each other. Now, we can express R s by considering θ small, and so we get the following approximate expression Note that for θ = 0 , we have the shadow radius for the Schwarzschild black hole case. Therefore, we notice that the shadow radius is reduced when we change the parameter θ . In Fig. 6, we see the circles that represent the shadow boundaries of the noncommutative black hole for different values of . Note that we have a reduction (56) (55), we obtain a non-zero result for the shadow radius, that is where M min = √ θ/π is the minimal mass 60 . Therefore, at the limit of M → 0 the shadow radius is proportional to the minimum mass and the black hole becomes a black hole remnant. We have shown this behavior in Fig. 7. In Fig. 7, we show the behavior of the shadow radius by keeping fixed and assuming small values of M. In Fig. 8, We show the behavior of the shadow radius by keeping M fixed and assuming small values of .

Conclusions
In summary, in this work, we investigate the quasinormal frequencies for a noncommutative Schwarzschild black hole by two different methods in order to investigate and compare the results. Using the sixth-order WKB approximation and Leaver's continuous fraction, we found that there is a small difference between the quasinormal frequencies obtained by each method mainly for small multipoles. The effects of the noncommutative parameter cause an increase in the real part of the quasinormal frequencies, while the magnitude of the imaginary part begins to grow and then decreases. For the black hole shadow we use the results obtained by  www.nature.com/scientificreports/ the WKB method to verify that in large l regimes the real part of quasinormal modes is inversely proportional to the shadow radius. In addition, we have shown that the shadow radius is non-zero at the zero mass limit. Therefore being proportional to a minimum mass. However for θ = 0 , we recover the shadow radius for the Schwarzschild black hole case. Finally, we also notice that the shadow radius is reduced when we increase the noncommutative parameter.